The upper main sequence in h and chi Persei
Abstract
Binary interactions play a crucial role in the evolution and eventual outcomes of massive stars. Rich young open clusters provide large coeval populations to constrain the effects of binary evolution. The Double Cluster, with a turn-off mass well above the threshold for core-collapse supernovae, is an excellent test bed for these processes. We used h and chi Persei, together with NGC 663, to constrain the evolutionary pathways of massive stars, particularly the role of binary interaction. We present spectroscopy of around 80 stars to obtain spectral types and derive stellar parameters. We combined this dataset with Gaia astrometry to evaluate their evolutionary status and possible evolutionary paths. We derived atmospheric parameters for almost 60 stars in the upper main sequence (B2V and earlier) and found broad agreement between two independent fully automated procedures. We identified the cluster turn-offs between B1 V and B1.5-2IV and differentiated this feature from the vicinity of theTAMS, where we found a population of B1-B1.5 giants, with a high fraction of Be stars. The bulk of the population in all of the massive clusters studied in the Perseus arm is consistent with single-star evolutionary models at a given age, but some B-type supergiants are much more luminous than any other cluster star. Their typical cluster kinematics and stellar parameters suggest a merger origin. Other lower-luminosity B-type supergiants seem consistent with the rest of the population. Kinematic analysis has indicated that most Be stars have not been dynamically perturbed by a supernova explosion. Those below the turn-off are likely to have been formed via case A mass transfer. The more massive Be stars above the turn-off do not display any other characteristic indicating a distinct evolutionary population (abridged)
Related
- The upper main sequence in h and ̧hi Persei
- Characterizing NGC 6383: Study of fundamental properties,pre-main sequence stars, mass segregation, and age using Gaia DR3 and 2MASS
- Super-Chandrasekhar white dwarfs by the evolution of magnetized main-sequence stars: New mass-limits from STARS simulation
- Super-Chandrasekhar White Dwarfs by the Evolution of Magnetized Main-sequence Stars: New Mass Limits from STARS Simulation
- Re-calibrated analytic stellar evolution formulae for the main sequence: Extension to massive stars and variations in [α/Fe]
BibTeX
@misc{marco2026upper,
title = {{The upper main sequence in h and chi Persei}},
author = {A. Marco and I. Negueruela and N. Castro and K. Rubke},
howpublished = {arXiv},
year = {2026},
month = nov,
doi = {10.48550/arxiv.2611.01160},
eprint = {2611.01160},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2611.01160},
}
RIS
TY - UNPB
TI - The upper main sequence in h and chi Persei
AU - A. Marco
AU - I. Negueruela
AU - N. Castro
AU - K. Rubke
PY - 2026
DA - 2026/11/01
PB - arXiv
DO - 10.48550/arxiv.2611.01160
UR - https://arxiv.org/abs/2611.01160
AB - Binary interactions play a crucial role in the evolution and eventual outcomes of massive stars. Rich young open clusters provide large coeval populations to constrain the effects of binary evolution. The Double Cluster, with a turn-off mass well above the threshold for core-collapse supernovae, is an excellent test bed for these processes. We used h and chi Persei, together with NGC 663, to constrain the evolutionary pathways of massive stars, particularly the role of binary interaction. We present spectroscopy of around 80 stars to obtain spectral types and derive stellar parameters. We combined this dataset with Gaia astrometry to evaluate their evolutionary status and possible evolutionary paths. We derived atmospheric parameters for almost 60 stars in the upper main sequence (B2V and earlier) and found broad agreement between two independent fully automated procedures. We identified the cluster turn-offs between B1 V and B1.5-2IV and differentiated this feature from the vicinity of theTAMS, where we found a population of B1-B1.5 giants, with a high fraction of Be stars. The bulk of the population in all of the massive clusters studied in the Perseus arm is consistent with single-star evolutionary models at a given age, but some B-type supergiants are much more luminous than any other cluster star. Their typical cluster kinematics and stellar parameters suggest a merger origin. Other lower-luminosity B-type supergiants seem consistent with the rest of the population. Kinematic analysis has indicated that most Be stars have not been dynamically perturbed by a supernova explosion. Those below the turn-off are likely to have been formed via case A mass transfer. The more massive Be stars above the turn-off do not display any other characteristic indicating a distinct evolutionary population (abridged)
ER -